Best observations in TeV----shell-type SNRsgive us more knowabout CRs acceleration----diffusive shock accelerationButelectronorhadron?A&A464bopcooApJ661（2007)120ApJ692（2009）W236(2007)2351001500D.E45.5100-39c28889200.64D.4Mes0.22040d00RX47.0.2.20J0852.0-4622RCW86RXPS09h00m08h50m14°45J1713m3946RA (hours)RightAscension(J2000)raXMMMAPSMOOTHEDHESS EXCESSMAPTOHESSPSFSN1006,X-50R3POrays,XMMskav41.8-41.842-42-42.2-42.2SN1006,VHEY-42.4-42.415h04m15hc2m15h04m15h02mRA (hours)XMMNEWTONRA(hours)2-4.5KEV
Best observations in TeV-shell-type SNRs give us more know about CRs acceleration-diffusive shock acceleration But electron or hadron?
轻子？强子？SNRRXJ1713.7-3946keV/TeV联合观测，A&A.449(2006)223-242A&A，464(2007)235-243(cS Ba) PINP B=7μG距离：1kpcB=9uG轻子模型39ASCA-B=11μG110ILL年龄：1600年EGRET+半径：1度Synchrotron10RadiationILLLICRadiation39.5OH.E.S.S流强（1TeV)：70%Crab10-12ATCA4010-13BremsstrahlungE.11101f10V10'101010'310510110°10PSFEnergy (eV)G-S,17h15m17h10mEGRETSbla) P/NP强子模型2101LmlLLLLnlLL1010101110121013109Energy (eV)
SNR RXJ1713.7-3946 keV/TeV联合观测，轻子？强子？ A&A，464(2007)235-243 轻子模型 强子模型 A&A. 449 (2006) 223-242 距离：1 kpc 年龄：1600 年 半径：1度 流强（1TeV）： 70%Crab
SNRRXJ1713.7-3946keV/TeV联合观测，+GeV观测，偏向于强子？A&A.449(2006)223-242A&A，464(2007)235-243(cS Ba) PINP B= 7μG距离：1kpcB=9uG轻子模型39ASCA-B=11μG110ILLLLL年龄：1600年EGRET+半径：1度Synchrotron10MLLLRadiationICRadiation39.5OUH.E.S.S流强（1TeV）：-70%Crab10-12ATCA4010-13Bremsstrahlung1110°10'10V101051010'310510310PSFEnergy (eV)?17h15m17h10m10-10EGRET30(-6op)(S us b1a) aPINaFermi初步结果ee251020Eregion (sre1)NEregion(src2)NEregion (src3)1510HE.S.S.deaoFemiLATtata10Simplerf decayInverse Compton (Pnrter et al)Prp+non-linear(Berezhko&yaelk10-135Esourcee101010121013109101014Energy (eV)348atic ongnuatf(deg)346
SNR RXJ1713.7-3946 keV/TeV联合观测，+GeV观测，偏向于强子？ A&A，464(2007)235-243 轻子模型 强子模型 A&A. 449 (2006) 223-242 Fermi 初步结果 距离：1 kpc 年龄：1600 年 半径：1度 流强（1TeV）： 70%Crab
The highest energies come from MILAGRO?CygnusregionMGROJ1908+06Dec=10c20Oae86J2019+371-J2032J1908-06TYO9070605030208040Galactic Longitude (degrees)Medianenergies~20TeV
New anisotropy component and corotation evidenceof the GCR (Science 314(2006)439-443)Intensity@E~300TeVCelestial Intensitymap (E~3TeV)New anisotropy componentAmp=0.16% w/o corotation;1997-20011.002a)Observation:0.03%+0.03%60(Bep)sod4020O0.9971.0066.9997A0003a(oeo2001-2005601.0041.0008D99921.002b)601.002(Bop)ooa0.9986tive.00144040200.9982000190.9981e0.996C.9970.99420.992sc)1997-20010501001502003502503001.00R.A. (deg)2001-2005z3ndt 14.6/180.999b)0.00032±0.00026Amp.0501001502002503003501.002R.A. (deg)259.9±46.5Significance (o)d)(Bep)e)(bep)404010o0.9982020050100150200250300350300310320330300310320330R.A. (deg)R.A (deg)R.A. (deg)
New anisotropy component and corotation evidence of the GCR (Science 314(2006)439-443) New anisotropy component Amp=0.16% w/o corotation; Observation: 0.03%±0.03%. Celestial Intensity map (E~3TeV) Intensity @ E~300TeV